Let $X$ be a compact Kahler manifold, and let $L$ be a line bundle on $X.$ Define $I_k(L)$ to be the kernel of the multiplication map $ Sym^k H^0 (L) o H^0 (L^k).$ For all $h leq k,$ we define a map $ ho : I_k(L) o Hom (H^{p,q} (L^{-h}), H^{p+1,q-1} (L^{k-h})).$ When $L = K_X$ is the canonical bundle, the map $ ho$ computes a second fundamental

SAO 85766 (b = +20o) is an IRAS source with far-infrared colours similar to planetary nebulae. According to the HDE catalogue, its spectrum in 1940 was that of an A5 star. The UV fluxes and colours derived from data obtained by the TD1 satellite in 1972 also indicate that SAO 85766 was an A-type supergiant at that epoch. However, high resolution

We study the effect of microturbulence in the line formation calculations of H and He lines, in the parameter range typical for O and early B stars. We are specially interested in its effect on the determination of stellar parameters: Teff, log g and specially on the He abundance. We first analyze the behaviour of H and He model lines between 4 000

We present a mechanism to produce X-ray transient periodic variations in AGN. This mechanism is triggered off by Compton scattering in the infalling plasma into a black hole, which can induce an electric charge in the singularity. The charging and discharging processes can affect the X-ray luminosity of AGN.

The dynamo model of solar magnetic field generation assumes that magnetic flux is retained at the dynamo site for times of the order of the solar-cycle period. However, flux tubes in the solar convection zone are expected to be buoyant, rising to the surface on timescales much shorter than the solar cycle. Since the initial 1955 paper by Parker on

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